Lack of late-accreted material as the origin of 182W excesses in the Archean mantle: Evidence from the Pilbara Craton, Western Australia

1Gregory J.Archer,1Gregory A.Brennecka,2 Philipp Gleißner,3Andreas Stracke,2Harry Becker,1Thorsten Kleine
Earth and Planetary Science Letters 528, 115841 Link to Article []
1Institut für Planetologie, University of Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany
2Institut für Geologische Wissenschaften, Freie Universität Berlin, Malteserstrasse 74-100, 12249 Berlin, Germany
3Institut für Mineralogie, University of Münster, Corrensstrasse 24, 48149 Münster, Germany
Copyright Elsevier

We report 182W and 142Nd isotopic compositions, 187Re–187Os systematics, and abundances of highly siderophile elements (HSE: Re, Os, Ir, Ru, Rh, Pt, Pd, and Au) for a suite of komatiites and basalts from the ∼3.3Ga Ruth Well Formation and the ∼3.45Ga Warrawoona Group of the Pilbara Craton, Western Australia. The 182W compositions from all samples are indistinguishable from each other, and more radiogenic than modern bulk silicate Earth, with a mean μ182W value of +9.1±4.2 (2SD). By contrast, the 142Nd values for all samples are indistinguishable from each other and terrestrial standards, with a mean μ142Nd value of −1.6±3.2 (2SD). The 146Sm–142Nd and 187Re–187Os systematics are consistent with chondritic Sm/Nd and Re/Os ratios in the mantle source during the lifetime of 182Hf, and the observed 182W excesses therefore cannot be accounted for by early Hf–W fractionation by magma ocean processes, neither by silicate liquid-crystal fractionation nor by high P–T metal-silicate equilibration. The estimated abundances of HSE in the mantle source, however, are significantly lower than modern bulk silicate Earth, with only 51±9% (1SD) of modern bulk silicate Earth abundances. These results are consistent with a partial lack of late-accreted material within the Pilbara source at ∼3.3Ga to account for the 182W excesses. Further, widespread 182W excesses of similar magnitude in other Archean mantle-derived rocks worldwide strongly suggests that a common process, most likely incomplete addition of late-accreted material, was responsible. The apparent mismatch between late-accreted 182W–HSE systematics for some other localities likely reflects either the inherent difficulties associated with estimating source HSE abundances, and/or dissociation of W and HSE by mantle processes. Finally, the combined average 182W–HSE systematics of Archean samples indicate that the pre-late accretion BSE likely had a μ182W value similar to that of the lunar mantle, which strongly suggests post-giant impact Earth–Moon equilibration and indicates that the Moon formed after 182Hf extinction.


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